Seismic constraints on rotation of Sun-like star and mass of exoplanet
Rotation is thought to drive cyclic magnetic activity in the Sun and Sun-like stars. Stellar dynamos, however, are poorly understood owing to the scarcity of observations of rotation and magnetic fields in stars. Here, inferences are drawn on the internal rotation of a distant Sun-like star by study...
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| creator | Gizon, Laurent Ballot, Jérome Michel, Eric Stahn, Thorsten Vauclair, Gérard Bruntt, Hans Pierre-Olivier Quirion Othman Benomar Vauclair, Sylvie Appourchaux, Thierry Auvergne, Michel Baglin, Annie Barban, Caroline Baudin, Fréderic Bazot, Michaël Campante, Tiago Catala, Claude Chaplin, William Creevey, Orlagh Deheuvels, Sébastien Dolez, Noël Elsworth, Yvonne García, Rafael Gaulme, Patrick Mathis, Stéphane Mathur, Savita Mosser, Benoît Régulo, Clara Roxburgh, Ian Salabert, David Samadi, Réza Sato, Kumiko Verner, Graham Hanasoge, Shravan Sreenivasan, Katepalli R |
| description | Rotation is thought to drive cyclic magnetic activity in the Sun and Sun-like stars. Stellar dynamos, however, are poorly understood owing to the scarcity of observations of rotation and magnetic fields in stars. Here, inferences are drawn on the internal rotation of a distant Sun-like star by studying its global modes of oscillation. We report asteroseismic constraints imposed on the rotation rate and the inclination of the spin axis of the Sun-like star HD 52265, a principal target observed by the CoRoT satellite that is known to host a planetary companion. These seismic inferences are remarkably consistent with an independent spectroscopic observation (rotational line broadening) and with the observed rotation period of star spots. Furthermore, asteroseismology constrains the mass of exoplanet HD 52265b. Under the standard assumption that the stellar spin axis and the axis of the planetary orbit coincide, the minimum spectroscopic mass of the planet can be converted into a true mass of 1.85 (+0.52,-0.42) M_Jupiter, which implies that it is a planet, not a brown dwarf. |
| doi_str_mv | 10.48550/arxiv.1308.4352 |
| format | Article |
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Stellar dynamos, however, are poorly understood owing to the scarcity of observations of rotation and magnetic fields in stars. Here, inferences are drawn on the internal rotation of a distant Sun-like star by studying its global modes of oscillation. We report asteroseismic constraints imposed on the rotation rate and the inclination of the spin axis of the Sun-like star HD 52265, a principal target observed by the CoRoT satellite that is known to host a planetary companion. These seismic inferences are remarkably consistent with an independent spectroscopic observation (rotational line broadening) and with the observed rotation period of star spots. Furthermore, asteroseismology constrains the mass of exoplanet HD 52265b. Under the standard assumption that the stellar spin axis and the axis of the planetary orbit coincide, the minimum spectroscopic mass of the planet can be converted into a true mass of 1.85 (+0.52,-0.42) M_Jupiter, which implies that it is a planet, not a brown dwarf.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1308.4352</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Brown dwarfs ; Dwarf planets ; Extrasolar planets ; Inclination ; Jupiter ; Line broadening ; Physics - Solar and Stellar Astrophysics ; Planetary orbits ; Rotating generators ; Rotational spectra ; Solar oscillations ; Solar rotation ; Spectroscopy ; Stellar magnetic fields ; Stellar oscillations ; Stellar rotation ; Stellar seismology</subject><ispartof>arXiv.org, 2013-08</ispartof><rights>2013. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27902</link.rule.ids><backlink>$$Uhttps://doi.org/10.1073/pnas.1303291110$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.1308.4352$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Gizon, Laurent</creatorcontrib><creatorcontrib>Ballot, Jérome</creatorcontrib><creatorcontrib>Michel, Eric</creatorcontrib><creatorcontrib>Stahn, Thorsten</creatorcontrib><creatorcontrib>Vauclair, Gérard</creatorcontrib><creatorcontrib>Bruntt, Hans</creatorcontrib><creatorcontrib>Pierre-Olivier Quirion</creatorcontrib><creatorcontrib>Othman Benomar</creatorcontrib><creatorcontrib>Vauclair, Sylvie</creatorcontrib><creatorcontrib>Appourchaux, Thierry</creatorcontrib><creatorcontrib>Auvergne, Michel</creatorcontrib><creatorcontrib>Baglin, Annie</creatorcontrib><creatorcontrib>Barban, Caroline</creatorcontrib><creatorcontrib>Baudin, Fréderic</creatorcontrib><creatorcontrib>Bazot, Michaël</creatorcontrib><creatorcontrib>Campante, Tiago</creatorcontrib><creatorcontrib>Catala, Claude</creatorcontrib><creatorcontrib>Chaplin, William</creatorcontrib><creatorcontrib>Creevey, Orlagh</creatorcontrib><creatorcontrib>Deheuvels, Sébastien</creatorcontrib><creatorcontrib>Dolez, Noël</creatorcontrib><creatorcontrib>Elsworth, Yvonne</creatorcontrib><creatorcontrib>García, Rafael</creatorcontrib><creatorcontrib>Gaulme, Patrick</creatorcontrib><creatorcontrib>Mathis, Stéphane</creatorcontrib><creatorcontrib>Mathur, Savita</creatorcontrib><creatorcontrib>Mosser, Benoît</creatorcontrib><creatorcontrib>Régulo, Clara</creatorcontrib><creatorcontrib>Roxburgh, Ian</creatorcontrib><creatorcontrib>Salabert, David</creatorcontrib><creatorcontrib>Samadi, Réza</creatorcontrib><creatorcontrib>Sato, Kumiko</creatorcontrib><creatorcontrib>Verner, Graham</creatorcontrib><creatorcontrib>Hanasoge, Shravan</creatorcontrib><creatorcontrib>Sreenivasan, Katepalli R</creatorcontrib><title>Seismic constraints on rotation of Sun-like star and mass of exoplanet</title><title>arXiv.org</title><description>Rotation is thought to drive cyclic magnetic activity in the Sun and Sun-like stars. Stellar dynamos, however, are poorly understood owing to the scarcity of observations of rotation and magnetic fields in stars. Here, inferences are drawn on the internal rotation of a distant Sun-like star by studying its global modes of oscillation. We report asteroseismic constraints imposed on the rotation rate and the inclination of the spin axis of the Sun-like star HD 52265, a principal target observed by the CoRoT satellite that is known to host a planetary companion. These seismic inferences are remarkably consistent with an independent spectroscopic observation (rotational line broadening) and with the observed rotation period of star spots. Furthermore, asteroseismology constrains the mass of exoplanet HD 52265b. 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Stellar dynamos, however, are poorly understood owing to the scarcity of observations of rotation and magnetic fields in stars. Here, inferences are drawn on the internal rotation of a distant Sun-like star by studying its global modes of oscillation. We report asteroseismic constraints imposed on the rotation rate and the inclination of the spin axis of the Sun-like star HD 52265, a principal target observed by the CoRoT satellite that is known to host a planetary companion. These seismic inferences are remarkably consistent with an independent spectroscopic observation (rotational line broadening) and with the observed rotation period of star spots. Furthermore, asteroseismology constrains the mass of exoplanet HD 52265b. 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| fulltext | fulltext |
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| language | eng |
| recordid | cdi_arxiv_primary_1308_4352 |
| source | Freely Accessible Journals; arXiv.org |
| subjects | Brown dwarfs Dwarf planets Extrasolar planets Inclination Jupiter Line broadening Physics - Solar and Stellar Astrophysics Planetary orbits Rotating generators Rotational spectra Solar oscillations Solar rotation Spectroscopy Stellar magnetic fields Stellar oscillations Stellar rotation Stellar seismology |
| title | Seismic constraints on rotation of Sun-like star and mass of exoplanet |
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